论文标题
超犯有电荷的物体和电子旋律对创建
Supercritically charged objects and electron-positron pair creation
论文作者
论文摘要
我们研究了基于Thomas-Fermi近似值的稳定性和$ e^+e^ - $成对的超批判性超重核，$ ud $ qm nuggets，strangelets和Strangeon掘金。模型参数是通过重现其质量和较早出版物中报告的质量和电荷属性来修复的。发现$ ud $ QM掘金，strangelets和strangeon掘金可能比$ {}^{56} $ fe稳定，分别分别分别为$ a \ gtrsim 315 $，$ 5 \ times10^4 $和$ 1.2 \ times10^8 $。对于那些反对中子排放稳定的人，最庞大的超级元素具有baryon number $ \ sim $ 965，而$ ud $ ud $ qm nuggets，strangelets和strangeon nuggets需要大于$ 39 $，433 $ 433和$ 2.7 \ times10^5 $。 $ e^+e^ - $ pair Creation将不可避免地开始使用充电数字的超核核，$ z \ geq177 $，$ ud $ ud $ qm QM nuggets，带有$ z \ geq163 $，ntrankelets，$ z \ geq 192 $，以及$ z \ geq 212 $的nuggets。通用关系$ q/r_e = \ left（m_e- \barμ_e\ right）/α$是在给定的电子化学势$ \barμ_e$的情况下获得的，其中$ q $是总费用，$ r_e $ r_e $ r_e $ the电子云的半径。这可以通过服用$ \barμ_e= -m_e $来预测最大充电数。对于具有$ \barμ_e<-m_e $的超判费用对象，$ e^+e^ - $对生产的衰减率是根据JWKB近似估算的。发现大多数主音以$ t \ Lessim 10^{ - 15} $ s排放，而对于具有$ r \ gtrsim 1000 $ fm的大对象，观察到持久的正电子排放。从超犯罪物体中的上音和歼灭可能部分负责二进制紧凑型恒星的合并，511 keV Continuum发射以及X射线光谱中的狭窄微弱发射线的合并期间的短$γ$ - 射线突发。
We investigate the stability and $e^+e^-$ pair creation of supercritically charged superheavy nuclei, $ud$QM nuggets, strangelets, and strangeon nuggets based on Thomas-Fermi approximation. The model parameters are fixed by reproducing their masses and charge properties reported in earlier publications. It is found that $ud$QM nuggets, strangelets, and strangeon nuggets may be more stable than ${}^{56}$Fe at $A\gtrsim 315$, $5\times10^4$, and $1.2\times10^8$, respectively. For those stable against neutron emission, the most massive superheavy element has a baryon number $\sim$965, while $ud$QM nuggets, strangelets, and strangeon nuggets need to have baryon numbers larger than $39$, 433, and $2.7\times10^5$. The $e^+e^-$ pair creation will inevitably start for superheavy nuclei with charge numbers $Z\geq177$, $ud$QM nuggets with $Z\geq163$, strangelets with $Z\geq 192$, and strangeon nuggets with $Z\geq 212$. A universal relation $Q/R_e = \left(m_e - \barμ_e\right)/α$ is obtained at a given electron chemical potential $\barμ_e$, where $Q$ is the total charge and $R_e$ the radius of electron cloud. This predicts the maximum charge number by taking $\barμ_e=-m_e$. For supercritically charged objects with $\barμ_e<-m_e$, the decay rate for $e^+e^-$ pair production is estimated based on the JWKB approximation. It is found that most positrons are emitted at $t\lesssim 10^{-15}$ s, while a long lasting positron emission is observed for large objects with $R\gtrsim 1000$ fm. The emission and annihilation of positrons from supercritically charged objects may be partially responsible for the short $γ$-ray burst during the merger of binary compact stars, the 511 keV continuum emission, as well as the narrow faint emission lines in X-ray spectra from galaxies and galaxy clusters.
